The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. I. Precise Spectral Types for 372 Stars

By R. O. Gray, P. Graham, S. R. Hoyt. 2000

209 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/09db4d935348b93d7790504eb3a022641e1d3909

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Citations in the corpus

Galaxy And Mass Assembly (GAMA): Spectroscopic analysis (2013, methodology): “The spectrum of each standard star is spectrally typed by comparing it to a set of theoretical spectra generated from Kurucz model atmospheres (Kurucz 1992), using the spectral synthesis code SPECTRUM (Gray & Corbally 1994; Gray et al. 2001).”
The star formation history and accretion-disc fraction among the K-type members of the Scorpius–Centaurus OB association (2016, background): “The spectral classification surveys of bright stars undertaken by Gray and collaborators (Gray et al. 2001, 2003, 2006) are based on the last generations of Morgan’s and Keenan’s hot and cool star spectral sequences (Morgan et al. 1978, Keenan & McNeil 1989) which are in common modern use.”
Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I. (2003, methodology): “…overshoot), and the synthetic spectra are computed with the spectral synthesis program SPECTRUM (Gray &Corbally 1994).3 Since the publication of the Gray et al. (2001) paper, much effort has been put into improving the spectral line list used by SPECTRUM, including updating the oscillator…”
SPECTROSCOPIC ORBITS FOR 15 LATE-TYPE STARS (2016, background): “While Cowley & Bidelman (1979) classified HD212754 as F7V, both Abt (1985) and Gray et al. (2001) gave it a spectral type of F8IV–V.”
INTRINSIC COLORS, TEMPERATURES, AND BOLOMETRIC CORRECTIONS OF PRE-MAIN-SEQUENCE STARS (2013, background): “Another example is σ Boo (HR 5447), which was considered a F2V standard by Morgan et al. (1943) and Johnson & Morgan (1953), but two later studies found the star to appear spectrally metal poor (F3V vw; Barry 1970) and (F4V kF2 mF1; Gray et al. 2001b).”
Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems (2014, background): “For reference, a typical value for dwarfs and subgiants is around 1 − 1.5 km s−1, going up to 2 − 2.5 km s−1 for stars on the red-giant branch (RGB), and possibly as high as 5 km s−1 in supergiants (e.g., Nissen 1981; Gray et al. 2001; Allende Prieto et al. 2004; Roederer & Sneden 2011).”
THE INFRARED TELESCOPE FACILITY (IRTF) SPECTRAL LIBRARY: COOL STARS (2009, methodology): “For F stars, we supplemented the lists generated from the aforementioned references with stars whose spectral types are given by Gray & Garrison (1989), Gray et al. (2001), and Abt & Morrell (1995).”
STELLAR DIAMETERS AND TEMPERATURES. III. MAIN-SEQUENCE A, F, G, AND K STARS: ADDITIONAL HIGH-PRECISION MEASUREMENTS AND EMPIRICAL RELATIONS (2013, unknown): “…(1979), (12) Jensen (1981), (13) Abt (1981), (14) Bouw (1981), (15) Abt (1985), (16) Abt (1986), (17) Gray (1989), (18) Gray & Garrison (1989a), (19) Gray & Garrison (1989b), (20) Keenan & McNeil (1989), (21) Abt & Morrell (1995), (22) Gray et al. (2001), (23) Gray et al. (2003), (24) Gray…”